Charge transfer between oxygen atoms and O<sup>+</sup>and H<sup>+</sup>ions

Stebbings, R. F.; Smith, A. C. H.; Ehrhardt, H.

doi:10.1029/jz069i011p02349

Cited by 174 publications

(98 citation statements)

References 13 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In Fig. 3 the new QMOCC computations are compared to the experiments of Stebbings et al (1964), Rutherford & Vroom (1974), Van Zyl & Stephen (1992), and Lindsay et al (1996), the QMOCC-FS calculations of Chambaud et al (1980), the QMOCC results of Kimura et al (1997), the electron nuclear dynamics (END) calculations of Hedström et al (1998), and the cross section deduced by detailed balance from the recommended reaction (1) cross section of Janev et al (1995). The current QMOCC is in good agreement with the experimental data for energies less than about 200 eV/u.…”

Section: Resultsmentioning

confidence: 99%

Charge transfer in collisions of O⁺ with H and H⁺ with O

Stancil

Schultz

Kimura

et al. 1999

Astron. Astrophys. Suppl. Ser.

113

103

View full text Add to dashboard Cite

Abstract. Cross sections and rate coefficients for total and fine-structure resolved charge transfer in collisions of O + with H and H + with O are presented for collision energies between 0.1 meV/u and 10 MeV/u and temperatures between 10 and 10 7 K. The results are obtained utilizing new quantal and semiclassical molecular-orbital closecoupling, classical trajectory Monte Carlo, and continuum distorted wave calculations in conjunction with previous experimental and theoretical data. Applications to various astrophysical and atmospheric environments are discussed.

show abstract

Section: Resultsmentioning

confidence: 99%

Charge transfer in collisions of O⁺ with H and H⁺ with O

Stancil

Schultz

Kimura

et al. 1999

Astron. Astrophys. Suppl. Ser.

113

103

View full text Add to dashboard Cite

show abstract

“…We use model cross sections derived from results given by Stebbings et al (1964). For nonresonant reactions ((H + , O) and (O + , H)) the cross sections are assumed to be constant while for resonant reactions ((H + , H) and (O + , O)) their dependency with respect to the relative velocity of the two particles is retained.…”

Section: Ionization Processesmentioning

confidence: 99%

Influence of the solar EUV flux on the Martian plasma environment

Modolo¹,

Chanteur²,

et al. 2005

View full text Add to dashboard Cite

Abstract. The interaction of the solar wind with the Martian atmosphere and ionosphere is investigated by using threedimensional, global and multi-species hybrid simulations. In the present work we focus on the influence of the solar EUV flux on the Martian plasma environment by comparing simulations done for conditions representative of the extrema of the solar cycle. The dynamics of four ionic species (H + , He ++ , O + , O + 2 ), originating either from the solar wind or from the planetary plasma, is treated fully kinetically in the simulation model in order to characterize the distribution of each component of the plasma, both at solar maximum and at solar minimum. The solar EUV flux controls the ionization frequencies of the exospheric species, atomic hydrogen and oxygen, as well as the density, the temperature, and thus the extension of the exosphere. Ionization by photons and by electron impacts, and the main charge exchange reactions are self-consistently included in the simulation model. Simulation results are in reasonable agreement with the observations made by Phobos-2 and Mars Global Surveyor (MGS) spacecraft: 1) the interaction creates a cavity, void of solar wind ions (H + , He ++ ), which depends weakly upon the phase of the solar cycle, 2) the motional electric field of the solar wind flow creates strong asymmetries in the Martian environment, 3) the spatial distribution of the different components of the planetary plasma depends strongly upon the phase of the solar cycle. The fluxes of the escaping planetary ions are computed from the simulated data and results for solar maximum are compared with estimates based on the measurements made by experiments ASPERA and TAUS on board Phobos-2.

show abstract

“…In addition, in the unperturbed interstellar medium one can rely on a charge exchange equilibrium of closely coupled O-and H-species yielding the fact Stebbings et al, 1964). Introducing the ionization degrees ξ H,O we thus find that the relation …”

Section: General Interaction Concept and Theoretical Approachmentioning

confidence: 97%

Imprints of a heliospheric bowshock on interstellar oxygen populations

Bzowski

Fahr

Grzędzielski

2006

Astrophys. Space Sci. Trans.

View full text Add to dashboard Cite

Abstract.It is well known that the nearby interstellar medium represents a partially ionized gas composed by different chemical species, amongst them hydrogen, helium and oxygen as the most abundant elements. While the passage of the interstellar protons and H-atoms over the solar system has been satisfactorily well modelled meanwhile, the entrance into the heliosphere of the other interstellar chemical species needs some additional care. Here we especially follow with Boltzmann-kinetic treatments the phase-space history of interstellar oxygen ions and atoms at their passage over the outer heliospheric bowshock and at their further approach towards the inner heliosphere. We describe the nose region of the bowshock as a mild MHD shock of a nearly perpendicular type. While the O-atoms pass over this shock with no velocity-space imprints, by contrast the O + -ions run over the shock structure with a typical overshoot velocity and on the downstream region are then picked up by the frozen-in magnetic fields that comove with the plasma bulk flow, i.e. the proton bulk flow. This leads to a strongly non-relaxated O-ion velocity distribution which substantially differs both from the local O-atom and proton distribution functions. Due to a strong charge exchange coupling between O-ions/atoms and H-atoms/ions the distributions downstream from the bowshock undergo permanent changes which we estimate in this study here. Even though relaxation processes operate by Coulomb collisions, wave-particle interactions and elastic atom-atom collisions, the bowshock imprints on the O-ion and atoms distribution functions may be conserved throughout the whole heliospheric interface, and, as we are going to suggest in this paper, in fact as such may be used as tracers to the physics and the nature of the bowshock. One of the main conclusions is that the population of O-atoms created in the vicinity of the bow-shock should carry a signature of the effective shock strength that could be detectable if the LIC magnetic field is about 2 microgauss or stronger.

show abstract

Charge transfer between oxygen atoms and O⁺and H⁺ions

Cited by 174 publications

References 13 publications

Charge transfer in collisions of O⁺ with H and H⁺ with O

Charge transfer in collisions of O⁺ with H and H⁺ with O

Influence of the solar EUV flux on the Martian plasma environment

Imprints of a heliospheric bowshock on interstellar oxygen populations

Contact Info

Product

Resources

About

Charge transfer between oxygen atoms and O+and H+ions

Cited by 174 publications

References 13 publications

Charge transfer in collisions of O+ with H and H+ with O

Charge transfer in collisions of O+ with H and H+ with O

Influence of the solar EUV flux on the Martian plasma environment

Imprints of a heliospheric bowshock on interstellar oxygen populations

Contact Info

Product

Resources

About

Charge transfer between oxygen atoms and O⁺and H⁺ions

Charge transfer in collisions of O⁺ with H and H⁺ with O

Charge transfer in collisions of O⁺ with H and H⁺ with O